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Simon, N.R., and R.B. Stothers, 1970: Evolution of very massive stars with pulsational mass loss. Astron. Astrophys., 6, 183-192.
Evolution with moderate mass loss has been investigated for hydrogen-burning stars whose mass exceed the critical mass for pulsational stability at the top of the main sequence. A prescription baaed on minimizing the degree of pulsational instability is used to specify the rate of mass loss. With a zero-age hydrogen abundance of X = 0.70 and electron-scattering opacity, stars of initially 60-115 M☉ become stable before the end of hydrogen burning; more massive stars evolve into unstable pure-helium stars of high mass. The smallest remnant left after hydrogen burning is 12 M☉, for an initial mass of 115 M☉. The hydrogen-burning tracks stay close to the zero-age main sequence, and the mass-loss rate is remarkably uniform, 3×l0-5 M☉/year. The helium burning phase is considered for the remnants of initially 100 and > 115 M☉. In contrast with the possible cases of no significant mass loss or very rapid mass loss, the assumption of moderate mass loss seems to yield results which are consistent with the relevant observational data, particularly for the most luminous group of Wolf-Rayet stars.
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